Measuring interstellar delays of PSR J0613−0200 over 7 yr, using the Large European Array for Pulsars. Issue 1 (28th September 2020)

• Record Type: Journal Article
• Authors: Main, R A; Sanidas, S A; Antoniadis, J; Bassa, C; Chen, S; Cognard, I; Gaikwad, M; Hu, H; Janssen, G H; Karuppusamy, R; Kramer, M; Lee, K J; Liu, K; Mall, G; McKee, J W; Mickaliger, M B; Perrodin, D; Stappers, B W; Tiburzi, C; Wucknitz, O; Wang, L; Zhu, W W
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 499:Issue 1(2020)
• Page Start: 1468
• Page End: 1479
• Publication Date: 2020-09-28
• Subjects: pulsars: general -- pulsars: individual: PSR J0613−0200; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2955
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Using data from the Large European Array for Pulsars, and the Effelsberg telescope, we study the scintillation parameters of the millisecond pulsar PSR J0613−0200 over a 7 yr timespan. The 'secondary spectrum' – the 2D power spectrum of scintillation – presents the scattered power as a function of time delay, and contains the relative velocities of the pulsar, observer, and scattering material. We detect a persistent parabolic scintillation arc, suggesting scattering is dominated by a thin, anisotropic region. The scattering is poorly described by a simple exponential tail, with excess power at high delays; we measure significant, detectable scattered power at times out to ${\sim}5 \, \mu {\rm s}$, and measure the bulk scattering delay to be between 50 to 200 ns with particularly strong scattering throughout 2013. These delays are too small to detect a change of the pulse profile shape, yet they would change the times of arrival as measured through pulsar timing. The arc curvature varies annually, and is well fitted by a one-dimensional scattering screen ${\sim}40{{\ \rm per\ cent}}$ of the way towards the pulsar, with a changing orientation during the increased scattering in 2013. Effects of uncorrected scattering will introduce time delays correlated over time in individual pulsars, and may need to be considered in gravitational wave analyses. Pulsar timing programmes would benefit from simultaneously recording in a way that scintillation can be resolved, in order to monitor the variable time delays caused by multipath propagation.